Other
Scientific paper
May 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aas...188.1705r&link_type=abstract
American Astronomical Society, 188th AAS Meeting, #17.05; Bulletin of the American Astronomical Society, Vol. 28, p.848
Other
Scientific paper
The W3 molecular cloud core has been observed with the BIMA and NRAO 12 m telescopes in the (13) CO (J = 1--0) and (J = 1--0) lines. Two BIMA fields were imaged, centered on the two infrared sources IRS 5 and IRS 4 (80('') west of IRS 5). The total masses of the the molecular cores associated with IRS 4 and IRS 5 are 1700 and 1100 M_sun, respectively. Seven clumps between 0.11 and 0.33 pc in size are identified with H_2 column densities in the range 1.3 to 2.1 x 10(23) cm(-2) . Derived masses are between 120 and 480 M_sun; under simple geometrical assumptions, n(H_2) is between 1.8 to 4.5 x 10(5) cm(-3) . For both cores the sum of all the individual clumps was about half of the total mass. The virial masses of the clumps ranged from 80 to 660 M_sun. The virial masses are near the measured H_2 masses. Comparisons of the (13) CO and C(18) O line strengths provide an estimate of the optical depth in (13) CO, assuming the C(18) O line has a negligible opacity. For two clumps located at IRS 5 and 20('') south of IRS 4 an opacities derived were 0.3 and 0.7, respectively. At the positions of IRS 4 and IRS 5, clumps are observed; the IRS 4 clump in particular has a n(H_2) about a factor of two larger than the other clumps. At the position of IRS 5, the data show a systematic velocity structure suggestive of rotation. A Keplarian velocity field was fitted to the data, which yielded a dynamical mass of 100 M_sun. Integrating the emission from the same clump over the same velocity range gives a H_2 masss of 110 M_sun. Using the derived H_2 column density toward IRS 5 and a previous HI Zeeman result, we can derive the ratio |B|/N_H (which is proportional to the magnetic flux-to-mass ratio, Phi /H_H) can be derived. The determined ratio is near the magnetically critical value, which is consistent with the standard theory of high mass star formation.
Crutcher Richard M.
Roberts Daniel A.
Troland Thomas H.
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